The geometry of accretion onto forming gas giants is an open question.
In the classical, simplified picture of accreting gas giants,
matter begins at a finite starting radius \({R_{\textnormal {acc}}}\)  and falls freely onto the planet
in a spherically symmetric fashion (e.g. [1]}, [2]}, [3]}, [4]}, [5]}, [6]}).
Based on the arguments in, for exmaple, [7]}, may be a reasonable model, at least on the scale of the Bondi radius \({R_{\textnormal {Bondi}}}\)  for sub-thermal planets,
that is, for planets whose Hill radius \({R_{\textnormal {Hill}}}=a(M_{\mathrm {p}}/3{M_{\star }})^{1/3}\) 
is smaller than the pressure scale height of the circumstellar disc (CSD),
with \(a\)  the semi-major axis and \({M_{\star }}\)  the stellar mass.
